Oxygen ions at Titan's exobase in a Voyager 1-type interaction from a hybrid simulation

Details Oxygen ions at Titan's exobase in a Voyager 1-type interaction from a hybrid simulation Oxygen ions at Titan's exobase in a Voyager 1-type interaction from a hybrid simulation

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jgra..11212205s&link_type=abstract

Journal of Geophysical Research, Volume 112, Issue A12, CiteID A12205

Physics

Plasma Physics

12

Planetary Sciences: Comets And Small Bodies: Magnetospheres (2756), Planetary Sciences: Solar System Objects: Titan, Space Plasma Physics: Kinetic And Mhd Theory, Planetary Sciences: Comets And Small Bodies: Ionospheres (2459)

Scientific paper

Titan's extensive atmosphere and exosphere interact with Saturn's rotating magnetospheric flow. We have studied this interaction with an advanced hybrid simulation model which employs a realistic ion composition in the upstream flow (subsonic O+and H+) and has improved spatial resolution. We present results for both the general characteristics of the interaction and the behavior of the O+flow ions near the exobase for the conditions during the Voyager 1 flyby. Our model shows that the ionotail and the magnetotail bend in a direction opposite to the convection electric field. This is validated with the total force on the incident flow species derived from basic plasma equations. We also present a simulated impact map for the oxygen ions of the flow with total O+precipitation rate 1.3 × 1024 s-1 at Titan's exobase. Although this rate indicates that the plasma conditions above the exobase do not inhibit O+precipitation on the exobase, the direction of the O+flow is shown to turn drastically near the exobase. The energy deposition of the medium-weight flow ions (such as O+) thus seems to be orders of magnitude larger than the energy deposition by pickup ions formed near Titan. However, the lightweight flow ions (H+) are effectively deflected by the magnetic barrier formed around Titan.

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